The changing face of RE J1034+396

Matthew Middleton

Spectral and timing similarities of AGN and BHB

A simple scaling...

Index of -1.35 from analytical method (Vaughan et al. 2005) and large scale simulations (Middleton & Done 2010)

Very ‘hot disc’ SED and massive soft excess

A simple scaling...

2 important things to do:

Try and determine the BHB analogy

Try and spot the QPO again

Unify physics

Determine duty cycle

A simple scaling...

Scaling gives 0.3-0.5LEdd

AGN seen with this but not same SED

Mass scaling with frequency >10LEdd

XRBs show LFQPO sub-Edd

1. Determining the analogy

‘3’ possibilities for soft excess spectrum:

1. Extra soft component 3. Smeared reflection

2. Smeared absorption

1. Determining the analogy

1. Determining the analogy

Need to select same components to account for disc stability

1. Determining the analogy

AGN QPO 67Hz QPO

1. Determining the analogy

First non-stationary AGN PSD!

2. Do we see it again??

Drop in rms consistent with difference in PSD normalisations.

Expect low T component to be more dominant at low energies in flux spectrum IF assumed deconvolution is a good description.

2. Do we see it again??

CompTT/nthcomp = 2.6

CompTT/nthcomp = 5.1

2. Do we see it again??

Conclusions...

1. By comparing the spectra and variability properties of REJ1034+396 we predict the likely spectral form is low T comp and high T comp

2. This appears similar to that of GRS1915+105 and bandpass correction leads to very similar power spectra

3. In the latest observation the QPO is not present

4. This gives the first non-stationary AGN PSD and shows transient nature much like the 67Hz QPO.

5. The power spectra and rms show much less variability and the spectral changes confirm our prediction of the deconvolution